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The Formation and Depletion of Molecules in Dense Interstellar Clouds
Abstract
The rates of a number of homogeneous gas phase reactions likely to occur in dense interstellar clouds composed primarily of molecular hydrogen are considered. Over 100 reactions are included; of these, more than half have known rate constants. These reactions are sufficient to produce and destroy polyatomic species such as H2O, HCN, NH3, and H2CO. Steady-state abundances of about 35 species are calculated for clouds of density 1 0 < < 106 cm -3. Calculations are performed for cosmic-ray-induced ionization rates H3 = 10-17 and 10-18 1 Typical times for reaching steady-state (flH2 = 10 cm - 3, H3 = 10-17 s-1) vary for different species; e.g., H2 + 0.05 day, H3 + 0.3 year, 1130 3 x 10 years. Comparisons of calculated and observed column densities are presented for a number of regions. Subject headings: excitation and ionization - molecules, interstellar - nebulae
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Cited by
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Metadata
- Authors
- Herbst, E., & Klemperer, W.
- Venue
- The Astrophysical Journal
- Publisher
- American Astronomical Society
- Published
- 1973-10
- Volume
- 185
- Pages
- 505
- ISSN
- 0004-637X (ISSN-L)
- 1538-4357
- OpenAlex
- W2062151060
- Cited by
- 1,087
- References
- 0
- FWCI
- 20.61
- Type
- journal article
- Language
- en
- Open access
- closed
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- Herbst, E., & Klemperer, W. (1973). The Formation and Depletion of Molecules in Dense Interstellar Clouds. The Astrophysical Journal. https://doi.org/10.1086/152436
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